The Heppner‐Maynard Boundary measured by SuperDARN as a proxy for the latitude of the auroral oval. Issue 2 (12th February 2013)

• Record Type: Journal Article
• Authors: Imber, S. M.; Milan, S. E.; Lester, M.
• Is Part Of: Journal of geophysical research. Volume 118:Issue 2(2013:Feb.)
• Page Start: 685
• Page End: 697
• Publication Date: 2013-02-12
• Subjects: expanding/contracting polar cap -- SuperDARN -- IMAGE; Magnetospheric physics -- Periodicals; Space environment -- Periodicals; Cosmic physics -- Periodicals; Planets -- Atmospheres -- Periodicals; Heliosphere (Astrophysics) -- Periodicals; Geophysics -- Periodicals; 523.01
• DOI: 10.1029/2012JA018222
• Languages: English
• ISSNs: 2169-9380

Abstract

Abstract : [1] We present a statistical study relating the latitude of the auroral oval measured by the Imager for Magnetopause‐to‐Aurora Global Exploration (IMAGE) SI‐12 proton auroral camera to that of the Heppner‐Maynard Boundary (HMB) determined from Super Dual Auroral Radar Network (SuperDARN) data during the period 2000–2002. The HMB represents the latitudinal extent of the ionospheric convection pattern. The oval latitude from the proton auroral images is determined using the method of Milan et al . (2009a), which fits a circle centered on a point 2° duskward and 5° antisunward of the magnetic pole. The auroral latitude at midnight is determined for those images where the concurrent SuperDARN northern hemisphere maps contain more than 200 data points such that the HMB is well‐defined. The statistical study comprises over 198, 000 two‐minute intervals, and we find that the HMB is located on average 2.2° equatorward of the proton auroral latitude. A superposed epoch analysis of over 2500 substorms suggests that the separation between the HMB and the oval latitude increases slightly during periods of high geomagnetic activity. We suggest that during intervals where there are no auroral images available, the HMB latitude and motion could be used as a proxy for that of the aurora, and therefore provide information about motions of the open/closed field line boundary. Key Points: Characterise HMB latitude distribution Compare HMB latitude with auroral latitude Dynamic motion of HMB follows auroral latitude